source: trunk/LMDZ.TITAN/deftank/callphys.def @ 1777

## Orbit / general options
## ~~~~~~~~~~~~~~~~~~~~~~~
# Run with or without tracer transport ?
tracer    = .false.
# Diurnal cycle ?  if diurnal=false, diurnally averaged solar heating
diurnal   = .true.
# Seasonal cycle ? if season=false, Ls stays constant, to value set in "start"
season    = .true. 
# Tidally resonant orbit ? must have diurnal=false, correct rotation rate in newstart
tlocked   = .false.
# Tidal resonance ratio ? ratio T_orbit to T_rotation
nres      = 1
# Write some more output on the screen ?
lwrite    = .false.
# Save statistics in file "stats.nc" ?
callstats = .false.
# Test energy conservation of model physics ?
enertest  = .true.
# check if cpp matches gases.def (should be false in 1d)
check_cpp_match = .false.
# force cpp and mugaz values from gases.def (should be false in 1d)
force_cpp = .false.

## Directory where external input files are
## ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
datadir     = ../../datagcm

## Radiative transfer options
## ~~~~~~~~~~~~~~~~~~~~~~~~~~
# call radiative transfer?
callrad    = .true.
# the rad. transfer is computed every "iradia" physical timestep
iradia     = 5
# Use blackbody for stellar spectrum ?
stelbbody    = .false.
# Stellar blackbody temperature ?
stelTbb      = 2000.000
# call multilayer correlated-k radiative transfer ?
corrk      = .true.
# folder in which correlated-k data is stored ?
  corrkdir   = 23x23_nocia_z55_T220
# call visible gaseous absorption in radiative transfer ?
callgasvis = .true.
# call continuum in radiative transfer ?
Continuum = .true.
# Allow temperatures above kmatrix tmax
strictboundcorrk = .false.
# Include Rayleigh scattering in the visible ?
rayleigh   = .true.
# Uniform absorption coefficient in radiative transfer?
graybody     = .false.
# Constant absorption coefficient in visible 
#      (in m^2/kg; only if graybody=true):
#      tau_surf= kappa*P/g
kappa_VI = 0.
# Constant absorption coefficient in IR
#      (in m^2/kg; only if graybody=true):
kappa_IR = 0.
# Use Newtonian cooling in place of radiative transfer ?
newtonian    = .false.
# Radiative timescale for Newtonian cooling ? [only if newtonian = T]
tau_relax    = 30.00000
# Test physics timescale in 1D ?
testradtimes = .false.
# Characteristic planetary equilibrium (black body) temperature
# This is used only in the aerosol radiative transfer setup. (see aerave.F)
tplanet    = 94.
# Output spectral OLR in 1D/3D?
specOLR    = .false.
# Output global radiative balance in file 'rad_bal.out' - slow for 1D!!
meanOLR    = .false.
# Remove lower boundary (e.g. for gas giant sims)
noradsurf    = .false. 

## Chemistry
## ~~~~~~~~~
# call chemistry ? (must have tracer=true)
callchim = .false.
# chemistry is computed every "ichim" phys. timestep
ichim = 20
# Activate zonal mean ? (must match callchim)
moyzon_ch = .false.

## Star type
## ~~~~~~~~~
startype = 1
# ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
# The choices are:
#
#       startype = 1            Sol        (G2V-class main sequence)
# ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
# Stellar flux at 1 AU. Examples:
# 1366.0 W m-2          Sol today
# 1024.5 W m-2          Sol today x 0.75 = weak early Sun
Fat1AU = 1366.0

## Tracer and aerosol options 
## ~~~~~~~~~~~~~~~~~~~~~~~~~~
# Gravitational sedimentation of tracers (just H2O ice for now) ?
sedimentation = .false.

## Other physics options
## ~~~~~~~~~~~~~~~~~~~~~
# call turbulent vertical diffusion ?
calldifv = .true.
# use turbdiff instead of vdifc ?
UseTurbDiff = .true.
# call convective adjustment ?
calladj  = .true.
# call thermal conduction in the soil ?
callsoil = .true.